Difference between revisions of "Summary LFI"

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[[File:Lfi_perf.jpg|thumb|center|655px|<math>^{ \rm a \, }</math> White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the withe noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data
 
[[File:Lfi_perf.jpg|thumb|center|655px|<math>^{ \rm a \, }</math> White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the withe noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data
 
<math>^{ \rm b \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{50mm} </math>
 
<math>^{ \rm b \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{50mm} </math>
 +
 
<math>^{ \rm c \, }</math> FWHM and ellipticity from effective beam evaluated as mean from different position on the sky. <math>\hspace{42mm} </math>
 
<math>^{ \rm c \, }</math> FWHM and ellipticity from effective beam evaluated as mean from different position on the sky. <math>\hspace{42mm} </math>
 
<math>^{ \rm d \, }</math> FWHM from effective beam evaluated as FWHM<math>_{eff} = \sqrt{\frac{Ω}{2π}} · 2 · \sqrt{2 \log 2}</math>, where Ω is the mean beam solid angle of the effective beam. Those are the values used in the source extraction pipeline {{BibCite|planck2013-p05}} {{P2013|28}}
 
<math>^{ \rm d \, }</math> FWHM from effective beam evaluated as FWHM<math>_{eff} = \sqrt{\frac{Ω}{2π}} · 2 · \sqrt{2 \log 2}</math>, where Ω is the mean beam solid angle of the effective beam. Those are the values used in the source extraction pipeline {{BibCite|planck2013-p05}} {{P2013|28}}

Revision as of 16:23, 4 July 2014

The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper [1]Planck-2013-II .


Table 1. Summary of the LFI performance parameters

[math]^{ \rm a \, }[/math] FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. [math]\hspace{480mm} [/math] [math]^{ \rm b \, }[/math] FWHM from effective beam estimated from the main beam solid angle of the effective beam. Those are the values used in the source extraction pipeline [2]Planck-2013-XXVIII . [math]{\hspace{35mm}}[/math] [math]^{ \rm c \, }[/math] White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the white noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data.


References[edit]

  1. Planck 2013 results: The Low Frequency Instrument data processing, Planck Collaboration 2013 II, A&A, in press, (2014).
  2. Planck 2013 results: The Planck Catalogue of Compact Sources, Planck Collaboration XXVIII, A&A, in press, (2014).

(Planck) Low Frequency Instrument

Full-Width-at-Half-Maximum